The helium abundance and the luminosity of the main-sequence F stars from uvby-beta photometric data

Details The helium abundance and the luminosity of the main-sequence F stars from uvby-beta photometric data The helium abundance and the luminosity of the main-sequence F stars from uvby-beta photometric data

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987azh....64..747s&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 64, July-Aug. 1987, p. 747-754. In Russian.

Astronomy and Astrophysics

Astronomy

2

Abundance, F Stars, Helium, Main Sequence Stars, Stellar Luminosity, Stellar Spectrophotometry, Ubv Spectra, Milky Way Galaxy, Spectrum Analysis, Stellar Envelopes, Stellar Structure

Scientific paper

The relation between the metallicity of F stars and their loci on the c1,β diagram is investigated for a sample of 2000 galactic-disk F stars having uvbyβ data. It is found that the lower envelope and the mean main sequence for stars with larger metallicities lie lower than those for the stars with lesser metallicities, though larger metallicity requires them to lie higher. The discrepancy is suggested to indicate the larger helium abundance in more metal-rich stars. The required difference in the Y value is found to be ΔY ≈ 0.1 if the disk stars constitute two discrete metallicity groups with z1 ≈ 0.01 and z2 ≈ 0.02. The authors conclude that the c1,β diagram for F stars gives evidence in favour of the discreteness of the actual metallicity distribution. It is shown that with increasing metallicity the helium abundance runs as ΔY ≈ 10 ΔZ (in contrast to the widely used relation ΔY ≈ 3 ΔZ).

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